PSP Bibliography


  • Clicking on the DOI link will open a new window with the original bibliographic entry from the publisher.
  • Clicking on a single author will show all publications by the selected author.
  • Clicking on a single keyword, will show all publications by the selected keyword.

On the utility of flux rope models for CME magnetic structure below 30 R$_\ensuremath\odot$

AuthorLynch, Benjamin; Al-Haddad, Nada; Yu, Wenyuan; Palmerio, Erika; Lugaz, No\;
KeywordsParker Data Used; magnetohydrodynamics (MHD); Solar corona; Coronal mass ejection (CME); magnetic flux rope; Parker Solar Probe (PSP); Astrophysics - Solar and Stellar Astrophysics; Physics - Space Physics
AbstractWe present a comprehensive analysis of the three-dimensional magnetic flux rope structure generated during the Lynch et al. (2019, ApJ 880:97) magnetohydrodynamic (MHD) simulation of a global-scale, 360 \textdegree -wide streamer blowout coronal mass ejection (CME) eruption. We create both fixed and moving synthetic spacecraft to generate time series of the MHD variables through different regions of the flux rope CME. Our moving spacecraft trajectories are derived from the spatial coordinates of Parker Solar Probe s past encounters 7 and 9 and future encounter 23. Each synthetic time series through the simulation flux rope ejecta is fit with three different in situ flux rope models commonly used to characterize the large-scale, coherent magnetic field rotations observed in a significant fraction of interplanetary CMEs (ICMEs). We present each of the in situ flux rope model fits to the simulation data and discuss the similarities and differences between the model fits and the MHD simulation s flux rope spatial orientations, field strengths and rotations, expansion profiles, and magnetic flux content. We compare in situ model properties to those calculated with the MHD data for both classic bipolar and unipolar ICME flux rope configurations as well as more problematic profiles such as those with a significant radial component to the flux rope axis orientation or profiles obtained with large impact parameters. We find general agreement among the in situ flux rope fitting results for the classic profiles and much more variation among results for the problematic profiles. We also examine the force- free assumption for a subset of the flux rope models and quantify properties of the Lorentz force within MHD ejecta intervals. We conclude that the in situ flux rope models are generally a decent approximation to the field structure, but all the caveats associated with in situ flux rope models will still apply (and perhaps moreso) at distances below 30R$_\ensuremath\odot$ . We discuss our results in the context of future PSP observations of CMEs in the extended corona.
Year of Publication2022
JournalAdvances in Space Research
Number of Pages1614-1640
Date Publishedsep